The precision of the flux calibration is limited by:
Having determined a reasonable response curve R, it can readily be used to flux-calibrate any point-source object spectrum, f_obj: Where F_std is in physical units (erg/) and f_std is in quasi-ADU.
This, divided into the tabulated flux, F_std, of the standard star, finally yields the response curve, R: This pipeline product can be further processed (which includes extinction correction, normalization for exposure time, binning and gain) into the normalized standard star spectrum, f_std. Responses Curves Flux Calibration of the dataĪ standard star measurement is processed by the pipeline into the flat-fielded, extracted and wavelength-calibrated result, p_std. If however an object has been observed in different setups and should ultimately be merged into one single result spectrum, it is very useful to have a correction for the instrument response slope. These extracted but uncalibrated data come in non-physical units ('quasi-ADU'), with their large-scale slope determined by the ratio of stellar and flat field spectral slopes.įor line profile studies this is sufficient.
If a master response curve exists (which depends on setting and epoch), the pipeline then does the final step, flux calibration. The UVES pipeline delivers extracted spectra which are debiased, flattened, background subtracted, wavelength calibrated and extracted. UVES Quality Control and Data Processing:: ECH Flux calibration mirror sites: PL (internal link) HQ
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